For studying the effects of these corruptions on the 21-cm signal recovery, the visibilities can either be imaged and post-processed or used directly for PS estimation. Imaging is performed using either CASA or WSCLEAN [1]}. These are standard imaging software used for imaging radio astronomical data. For power spectrum determination, we use a PS pipeline developed based on the delay spectrum technique [2]} and implements Equation REF , which is further averaged according to Equation REF , producing the 2D and 1D PS. The spherical averaging can be done using either all the k-modes or only those outside the wedge. In the presence of RFI flagging, it implements either CLEAN [3]} or LSSA [4]} algorithms to reduce oscillatory features introduced due to non-uniform data samples. This has been used in [5]} to provide upper limits on the post-EoR PS and [6]} to provide a comparison between the efficacy of different RFI mitigation methods. A systematic analysis of the performance of the whole pipeline along with the PS estimations has been presented in [7]}. They have compared the impact of systematics for signal recovery using different arrays under identical conditions of sky and foregrounds. The PS pipeline is currently being integrated with the main pipeline and will be publicly released after successful integration and testing.
